Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate

K. B. Webber; T. T. Hansen; J. L. Marshall; J. D. Simon; A. B. Pace; B. Mutlu-Pakdil; A. Drlica-Wagner; C. E. Martínez-Vázquez; M. Aguena; S. S. Allam; O. Alves; E. Bertin; D. Brooks; A. Carnero Rosell; J. Carretero; L. N. da Costa; J. De Vicente; P. Doel; I. Ferrero; D. Friedel; J. Frieman; J. García-Bellido; G. Giannini; D. Gruen; R. A. Gruendl; S. R. Hinton; D. L. Hollowood; K. Honscheid; K. Kuehn; J. Mena-Fernández; F. Menanteau; R. Miquel; R. L.C. Ogando; M. E.S. Pereira; A. Pieres; A. A. Plazas Malagón; E. Sanchez; B. Santiago; J. Allyn Smith; M. Smith; E. Suchyta; G. Tarle; C. To; N. Weaverdyck; B. Yanny

doi:10.3847/1538-4357/ad0385

Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate

K. B. Webber, T. T. Hansen, J. L. Marshall, J. D. Simon, A. B. Pace, B. Mutlu-Pakdil, A. Drlica-Wagner, C. E. Martínez-Vázquez, M. Aguena, S. S. Allam, O. Alves, E. Bertin, D. Brooks, A. Carnero Rosell, J. Carretero, L. N. da Costa, J. De Vicente, P. Doel, I. Ferrero, D. FriedelJ. Frieman, J. García-Bellido, G. Giannini, D. Gruen, R. A. Gruendl, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L.C. Ogando, M. E.S. Pereira, A. Pieres, A. A. Plazas Malagón, E. Sanchez, B. Santiago, J. Allyn Smith, M. Smith, E. Suchyta, G. Tarle, C. To, N. Weaverdyck, B. Yanny

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Abstract

We present a detailed chemical abundance analysis of the brightest star in the ultrafaint dwarf (UFD) galaxy candidate Cetus II from high-resolution Magellan/MIKE spectra. For this star, DES J011740.53-173053, abundances or upper limits of 18 elements from carbon to europium are derived. Its chemical abundances generally follow those of other UFD galaxy stars, with a slight enhancement of the α-elements (Mg, Si, and Ca) and low neutron-capture element (Sr, Ba, and Eu) abundances supporting the classification of Cetus II as a likely UFD. The star exhibits lower Sc, Ti, and V abundances than Milky Way (MW) halo stars with similar metallicity. This signature is consistent with yields from a supernova originating from a star with a mass of ∼11.2 M _⊙. In addition, the star has a potassium abundance of [K/Fe] = 0.81, which is somewhat higher than the K abundances of MW halo stars with similar metallicity, a signature that is also present in a number of UFD galaxies. A comparison including globular clusters and stellar stream stars suggests that high K is a specific characteristic of some UFD galaxy stars and can thus be used to help classify objects as UFD galaxies.

Original language	English
Article number	141
Journal	Astrophysical Journal
Volume	959
Issue number	2
DOIs	https://doi.org/10.3847/1538-4357/ad0385
State	Published - Dec 1 2023

Funding

This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. T.T.H acknowledges support from the Swedish Research Council (VR 2021-05556). Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).

Funders	Funder number
Brazilian Instituto Nacional de Ciência e Tecnologia
Collaborating Institutions in the Dark Energy Survey
Fermi Research Alliance, LLC	DE-AC02-07CH11359
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
Science and Technology Facilities Council of the United Kingdom
National Science Foundation	AST-1138766, AST-1536171
U.S. Department of Energy
Office of Science
High Energy Physics
Ohio State University
University of Chicago
National Centre for Supercomputing Applications
Seventh Framework Programme
Higher Education Funding Council for England
Engineering Research Centers	240672, 306478, 291329
European Commission
European Research Council
Deutsche Forschungsgemeinschaft
Generalitat de Catalunya
Ministério da Ciência, Tecnologia e Inovação
Conselho Nacional de Desenvolvimento Científico e Tecnológico	465376/2014-2
Vetenskapsrådet	VR 2021-05556
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Financiadora de Estudos e Projetos
Ministerio de Ciencia e Innovación	SEV-2016-0588, SEV-2016-0597, MDM-2015-0509, PGC2018-094773, PGC2018-102021, ESP2017-89838
Instituto Nacional de Ciência e Tecnologia para Excitotoxicidade e Neuroproteção
Ministry of Education and Science of Ukraine
European Regional Development Fund

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Webber, K. B., Hansen, T. T., Marshall, J. L., Simon, J. D., Pace, A. B., Mutlu-Pakdil, B., Drlica-Wagner, A., Martínez-Vázquez, C. E., Aguena, M., Allam, S. S., Alves, O., Bertin, E., Brooks, D., Carnero Rosell, A., Carretero, J., da Costa, L. N., De Vicente, J., Doel, P., Ferrero, I., ... Yanny, B. (2023). Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate. Astrophysical Journal, 959(2), Article 141. https://doi.org/10.3847/1538-4357/ad0385

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title = "Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate",

abstract = "We present a detailed chemical abundance analysis of the brightest star in the ultrafaint dwarf (UFD) galaxy candidate Cetus II from high-resolution Magellan/MIKE spectra. For this star, DES J011740.53-173053, abundances or upper limits of 18 elements from carbon to europium are derived. Its chemical abundances generally follow those of other UFD galaxy stars, with a slight enhancement of the α-elements (Mg, Si, and Ca) and low neutron-capture element (Sr, Ba, and Eu) abundances supporting the classification of Cetus II as a likely UFD. The star exhibits lower Sc, Ti, and V abundances than Milky Way (MW) halo stars with similar metallicity. This signature is consistent with yields from a supernova originating from a star with a mass of ∼11.2 M ⊙. In addition, the star has a potassium abundance of [K/Fe] = 0.81, which is somewhat higher than the K abundances of MW halo stars with similar metallicity, a signature that is also present in a number of UFD galaxies. A comparison including globular clusters and stellar stream stars suggests that high K is a specific characteristic of some UFD galaxy stars and can thus be used to help classify objects as UFD galaxies.",

author = "Webber, {K. B.} and Hansen, {T. T.} and Marshall, {J. L.} and Simon, {J. D.} and Pace, {A. B.} and B. Mutlu-Pakdil and A. Drlica-Wagner and Mart{\'i}nez-V{\'a}zquez, {C. E.} and M. Aguena and Allam, {S. S.} and O. Alves and E. Bertin and D. Brooks and {Carnero Rosell}, A. and J. Carretero and {da Costa}, {L. N.} and {De Vicente}, J. and P. Doel and I. Ferrero and D. Friedel and J. Frieman and J. Garc{\'i}a-Bellido and G. Giannini and D. Gruen and Gruendl, {R. A.} and Hinton, {S. R.} and Hollowood, {D. L.} and K. Honscheid and K. Kuehn and J. Mena-Fern{\'a}ndez and F. Menanteau and R. Miquel and Ogando, {R. L.C.} and Pereira, {M. E.S.} and A. Pieres and {Plazas Malag{\'o}n}, {A. A.} and E. Sanchez and B. Santiago and Smith, {J. Allyn} and M. Smith and E. Suchyta and G. Tarle and C. To and N. Weaverdyck and B. Yanny",

note = "Publisher Copyright: {\textcopyright} 2023. The Author(s). Published by the American Astronomical Society.",

year = "2023",

month = dec,

day = "1",

doi = "10.3847/1538-4357/ad0385",

language = "English",

volume = "959",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

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Webber, KB, Hansen, TT, Marshall, JL, Simon, JD, Pace, AB, Mutlu-Pakdil, B, Drlica-Wagner, A, Martínez-Vázquez, CE, Aguena, M, Allam, SS, Alves, O, Bertin, E, Brooks, D, Carnero Rosell, A, Carretero, J, da Costa, LN, De Vicente, J, Doel, P, Ferrero, I, Friedel, D, Frieman, J, García-Bellido, J, Giannini, G, Gruen, D, Gruendl, RA, Hinton, SR, Hollowood, DL, Honscheid, K, Kuehn, K, Mena-Fernández, J, Menanteau, F, Miquel, R, Ogando, RLC, Pereira, MES, Pieres, A, Plazas Malagón, AA, Sanchez, E, Santiago, B, Smith, JA, Smith, M, Suchyta, E, Tarle, G, To, C, Weaverdyck, N & Yanny, B 2023, 'Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate', Astrophysical Journal, vol. 959, no. 2, 141. https://doi.org/10.3847/1538-4357/ad0385

TY - JOUR

T1 - Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate

AU - Webber, K. B.

AU - Hansen, T. T.

AU - Marshall, J. L.

AU - Simon, J. D.

AU - Pace, A. B.

AU - Mutlu-Pakdil, B.

AU - Drlica-Wagner, A.

AU - Martínez-Vázquez, C. E.

AU - Aguena, M.

AU - Allam, S. S.

AU - Alves, O.

AU - Bertin, E.

AU - Brooks, D.

AU - Carnero Rosell, A.

AU - Carretero, J.

AU - da Costa, L. N.

AU - De Vicente, J.

AU - Doel, P.

AU - Ferrero, I.

AU - Friedel, D.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Giannini, G.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Hinton, S. R.

AU - Hollowood, D. L.

AU - Honscheid, K.

AU - Kuehn, K.

AU - Mena-Fernández, J.

AU - Menanteau, F.

AU - Miquel, R.

AU - Ogando, R. L.C.

AU - Pereira, M. E.S.

AU - Pieres, A.

AU - Plazas Malagón, A. A.

AU - Sanchez, E.

AU - Santiago, B.

AU - Smith, J. Allyn

AU - Smith, M.

AU - Suchyta, E.

AU - Tarle, G.

AU - To, C.

AU - Weaverdyck, N.

AU - Yanny, B.

PY - 2023/12/1

Y1 - 2023/12/1

N2 - We present a detailed chemical abundance analysis of the brightest star in the ultrafaint dwarf (UFD) galaxy candidate Cetus II from high-resolution Magellan/MIKE spectra. For this star, DES J011740.53-173053, abundances or upper limits of 18 elements from carbon to europium are derived. Its chemical abundances generally follow those of other UFD galaxy stars, with a slight enhancement of the α-elements (Mg, Si, and Ca) and low neutron-capture element (Sr, Ba, and Eu) abundances supporting the classification of Cetus II as a likely UFD. The star exhibits lower Sc, Ti, and V abundances than Milky Way (MW) halo stars with similar metallicity. This signature is consistent with yields from a supernova originating from a star with a mass of ∼11.2 M ⊙. In addition, the star has a potassium abundance of [K/Fe] = 0.81, which is somewhat higher than the K abundances of MW halo stars with similar metallicity, a signature that is also present in a number of UFD galaxies. A comparison including globular clusters and stellar stream stars suggests that high K is a specific characteristic of some UFD galaxy stars and can thus be used to help classify objects as UFD galaxies.

AB - We present a detailed chemical abundance analysis of the brightest star in the ultrafaint dwarf (UFD) galaxy candidate Cetus II from high-resolution Magellan/MIKE spectra. For this star, DES J011740.53-173053, abundances or upper limits of 18 elements from carbon to europium are derived. Its chemical abundances generally follow those of other UFD galaxy stars, with a slight enhancement of the α-elements (Mg, Si, and Ca) and low neutron-capture element (Sr, Ba, and Eu) abundances supporting the classification of Cetus II as a likely UFD. The star exhibits lower Sc, Ti, and V abundances than Milky Way (MW) halo stars with similar metallicity. This signature is consistent with yields from a supernova originating from a star with a mass of ∼11.2 M ⊙. In addition, the star has a potassium abundance of [K/Fe] = 0.81, which is somewhat higher than the K abundances of MW halo stars with similar metallicity, a signature that is also present in a number of UFD galaxies. A comparison including globular clusters and stellar stream stars suggests that high K is a specific characteristic of some UFD galaxy stars and can thus be used to help classify objects as UFD galaxies.

UR - http://www.scopus.com/inward/record.url?scp=85180565252&partnerID=8YFLogxK

U2 - 10.3847/1538-4357/ad0385

DO - 10.3847/1538-4357/ad0385

M3 - Article

AN - SCOPUS:85180565252

SN - 0004-637X

VL - 959

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 141

ER -

Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate

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